The CME associated with the filament eruption on March 15, 2015 was observed with the LASCO instrument.
As reported in [1]}, during the C2.6 class flare of March 14, 2015 a
small filament erupted (their Figure 1 (a), F4 filament) and there was a slow CME observed in
LASCO C2 field–of–view (FOV) at \(\sim \)  13:30 UT. The speed and the angular width of this CME was 208 kms\(^{-1}\)  and 160\(^{\circ }\) 
respectively.
By the push from jet 1, the F\(_1\)  filament eruption on March 15, 2015 produced a halo CME, visible in the LASCO C2 FOV at 01:48 UT.
The CME was visible up to 27 R\(_{\odot }\)  in the LASCO C3 FOV.
The running difference of the C2 and C3 coronagraph images are shown in Figure REF .
The white circle represents the solar disk occulted by the coronagraph. In the C2 images,
the running difference of SDO AIA 193 Å images are displayed inside the white circles for the same time.
The red and yellow arrows indicate the leading
edge of the CME in the LASCO C2 and C3 FOV respectively. The black arrow in the first image of the bottom panel points to the CME
from the same AR on March 14, 2015. According to the LASCO CDAW Catalog ([2]}) the average CME speed
was 719 kms\(^{-1}\)  and the acceleration was -9.0 ms\(^{-2}\) .
The mass and kinetic energy of the CME were 3.0\(\times 10^{16}\)  gram and 7.7 \(\times 10^{31}\)  ergs respectively. Moreover, [3]} reported the maximum CME speed was 1100 kms\(^{-1}\) .
In C3 the FOV the CME of March 14-15, 2015 interacted at 02:18 UT. [3]} considered the interaction
of these CMEs as the cause of the largest geomagnetic storm of solar cycle 24 on March 17, 2015.
